A new version of the energy-balance method - Determination of nebular optical depths and temperatures of central stars of planetary nebulae

Details A new version of the energy-balance method - Determination of nebular optical depths and temperatures of central stars of planetary nebulae A new version of the energy-balance method - Determination of nebular optical depths and temperatures of central stars of planetary nebulae

Aug 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...248..191k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 248, no. 1, Aug. 1991, p. 191-196.

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Optical Thickness, Planetary Nebulae, Stellar Temperature, Abundance, Astronomical Spectroscopy, Computational Astrophysics, Photoionization, Stellar Spectra, Planetary Nebulae: General, Stars: Temperatures Of

Scientific paper

In this paper we present a new version of the Energy-Balance method (EB2) that allows the simultaneous determination of the temperature of the central ionizing star and of the optical depth of the surrounding nebula. Input data to the new method are, as for the classical E-B method, the observed intensities of collisionally excited lines in the nebular spectrum, with the Hell 4686 recombination line as additional input parameter. Another difference is that we had to leave the analytical approach of the classical E-B method and rely on models of photoionized nebulae. As a result of our calculations, we present a set of diagnostic curves that can be used for the determination of the central star temperature and the nebular optical depth. We also discuss in detail the effect of changes in the model input parameters on our diagnostics diagrams. The main result is that the presented diagrams are rather unaffected by changing the input parameters within reasonable limits, and that the general features of the diagnostics curves are shaped by basic physical processes, not by the details of the adopted photoionization model.

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